This accretion-related emission in metal lines, `line veiling', has been observed in a number of accreting TTS [1]}, [2]}, [3]}. In some, the line veiling has been found to be dominant, among them RU Lup [3]}, [5]}. The authors compare the \(V\) -band photometric variability of the star with the variability of the veiling and find that the veiling is not correlated, or only weakly related, to the stellar brightness during states of high veiling. They argue that there are two sources of veiling: a continuous excess emission, and narrow emission lines filling-in the photospheric absorption lines, both related to the accretion shocks and foot-prints of the accretion funnels. Line emission becomes the dominant component for high-veiling states (\(r>2\) ). In this case, a change in veiling does not lead to a corresponding change in stellar brightness, as it would happen if the veiling was caused by continuous emission alone.
